An improved and generalized theory for the collisional evolution of Keplerian systems

1978 ◽  
Vol 58 (2) ◽  
pp. 477-519 ◽  
Author(s):  
K. A. H�meen-Anttila
Keyword(s):  
Keplerian Systems ◽  
Collisional Evolution

Asteroid collisional evolution

Icarus ◽  
1990 ◽  
Vol 87 (2) ◽  
pp. 391-402 ◽  
Author(s):  
A. Cellino ◽  
V. Zappalà ◽  
D.R. Davis ◽  
P. Farinella ◽  
P. Paolicchi
Keyword(s):  
Collisional Evolution

scholarly journals Collisional Evolution of the Inner Zodiacal Cloud

2021 ◽  
Vol 2 (5) ◽  
pp. 185 ◽  
Author(s):  
J. R. Szalay ◽  
P. Pokorný ◽  
D. M. Malaspina ◽  
A. Pusack ◽  
S. D. Bale ◽  
...  
Keyword(s):  
Zodiacal Cloud ◽  
Collisional Evolution

scholarly journals Normal Forms for Perturbed Keplerian Systems

2002 ◽  
Vol 180 (2) ◽  
pp. 471-519 ◽  
Author(s):  
Jesús Palacián
Keyword(s):  
Normal Forms ◽  
Keplerian Systems

Anatexis witnessed post-collisional evolution of the Dabie orogen, China

2017 ◽  
Vol 145 ◽  
pp. 278-296 ◽  
Author(s):  
Haijin Xu ◽  
Junfeng Zhang
Keyword(s):  
Dabie Orogen ◽  
Collisional Evolution

Collisional Evolution of Small-Body Populations

Asteroids III ◽  
2002 ◽  
pp. 545-558
Author(s):  
Donald R. Davis ◽  
Daniel D. Durda ◽  
Francesco Marzari ◽  
Adriano Campo Bagatin ◽  
Ricardo Gil-Hutton
Keyword(s):  
Small Body ◽  
Collisional Evolution

The Pyrenean orogen: pre-, syn-, and post-collisional evolution

2002 ◽  
Vol 08 ◽  
Author(s):  
Jaume Vergés ◽  
Manel Fernàndez ◽  
Albert Martìnez
Keyword(s):  
Collisional Evolution

scholarly journals Impactor Flux on the Pluto-Charon System

2009 ◽  
Vol 5 (S263) ◽  
pp. 98-101 ◽  
Author(s):  
Gonzalo C. de Elía ◽  
Romina P. Di Sisto ◽  
Adrián Brunini
Keyword(s):  
Size Distribution ◽  
Kuiper Belt ◽  
Primary Source ◽  
Mean Motion ◽  
Stability And Instability ◽  
The Stability ◽  
Mean Motion Resonance ◽  
Collisional Evolution

AbstractIn this work, we study the impactor flux on Pluto and Charon due to the collisional evolution of Plutinos.To do this, we develop a statistical code that includes catastrophic collisions and cratering events, and takes into account the stability and instability zones of the 3:2 mean motion resonance with Neptune. Our results suggest that if 1 Pluto-sized object is in this resonance, the flux of D = 2 km Plutinos on Pluto is ~4–24 percent of the flux of D = 2 km Kuiper Belt projectiles on Pluto. However, with 5 Pluto-sized objects in the resonance, the contribution of the Plutino population to the impactor flux on Pluto may be comparable to that of the Kuiper Belt. As for Charon, if 1 Pluto-sized object is in the 3:2 resonance, the flux of D = 2 km Plutinos is ~10–63 percent of the flux of D = 2 km impactors coming from the Kuiper Belt. However, with 5 Pluto-sized objects, the Plutino population may be a primary source of the impactor flux on Charon. We conclude that it is necessary to specify the Plutino size distribution and the number of Pluto-sized objects in the 3:2 Neptune resonance in order to determine if the Plutino population is a primary source of impactors on the Pluto-Charon system.

scholarly journals Direct imaging of irregular satellite discs in scattered light

2020 ◽  
Vol 492 (4) ◽  
pp. 5709-5720
Author(s):  
Loic Nassif-Lachapelle ◽  
Daniel Tamayo
Keyword(s):  
Near Infrared ◽  
Thermal Emission ◽  
Scattered Light ◽  
Semimajor Axis ◽  
Detection Methods ◽  
Direct Imaging ◽  
Irregular Satellites ◽  
Long Period ◽  
Wide Range ◽  
Collisional Evolution

ABSTRACT Direct imaging surveys have found that long-period super-Jupiters are rare. By contrast, recent modelling of the widespread gaps in protoplanetary discs revealed by Atacama Large Millimetre Array suggests an abundant population of smaller Neptune to Jupiter-mass planets at large separations. The thermal emission from such lower-mass planets is negligible at optical and near-infrared wavelengths, leaving only their weak signals in reflected light. Planets do not scatter enough light at these large orbital distances, but there is a natural way to enhance their reflecting area. Each of the four giant planets in our Solar system hosts swarms of dozens of irregular satellites, gravitationally captured planetesimals that fill their host planets’ spheres of gravitational influence. What we see of them today are the leftovers of an intense collisional evolution. At early times, they would have generated bright circumplanetary debris discs. We investigate the properties and detectability of such irregular satellite discs (ISDs) following models for their collisional evolution from Kennedy & Wyatt (2011). We find that the scattered light signals from such ISDs would peak in the 10–100 au semimajor axis range implied by ALMA, and can render planets detectable over a wide range of parameters with upcoming high-contrast instrumentation. We argue that future instruments with wide fields of view could simultaneously characterize the atmospheres of known close-in planets, and reveal the population of long-period Neptune–Jupiter mass exoplanets inaccessible to other detection methods. This provides a complementary and compelling science case that would elucidate the early lives of planetary systems.

scholarly journals Long‐Term Collisional Evolution of Debris Disks

2008 ◽  
Vol 673 (2) ◽  
pp. 1123-1137 ◽  
Author(s):  
Torsten Lohne ◽  
Alexander V. Krivov ◽  
Jens Rodmann
Keyword(s):  
Debris Disks ◽  
Collisional Evolution

Reduced 4D oscillators and orbital elements in Keplerian systems: Cushman–Deprit coordinates

2020 ◽  
Vol 132 (11-12) ◽  
Author(s):  
S. Ferrer ◽  
F. Crespo ◽  
J. L. Zapata
Keyword(s):  
Orbital Elements ◽  
Keplerian Systems
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